Hot and Turbulent Gas in Clusters

TL;DR

This study uses advanced simulations to explore the relationship between thermal and turbulent energies in galaxy cluster gas, revealing a roughly linear relation and insights into turbulence production in hot clusters.

Contribution

It introduces a novel method to estimate turbulence in galaxy clusters using adaptive Kalman filtering on simulation data, linking turbulence with thermal energy and cluster temperature.

Findings

Turbulent velocity dispersions scale with gas temperature with an exponent around 0.5.

Turbulence is weakly correlated with halo mass.

Turbulent Mach number increases with the mean temperature of the WHIM.

Abstract

The gas in galaxy clusters is heated by shock compression through accretion (outer shocks) and mergers (inner shocks). These processes additionally produce turbulence. To analyse the relation between the thermal and turbulent energies of the gas under the influence of non-adiabatic processes, we performed numerical simulations of cosmic structure formation in a box of 152 Mpc comoving size with radiative cooling, UV background, and a subgrid scale model for numerically unresolved turbulence. By smoothing the gas velocities with an adaptive Kalman filter, we are able to estimate bulk flows toward cluster cores. This enables us to infer the velocity dispersion associated with the turbulent fluctuation relative to the bulk flow. For halos with masses above $10^{13}\,M_\odot$, we find that the turbulent velocity dispersions averaged over the warm-hot intergalactic medium (WHIM) and the intracluster medium (ICM) are approximately given by powers of the mean gas temperatures with exponents around 0.5, corresponding to a roughly linear relation between turbulent and thermal energies and transonic Mach numbers. However, turbulence is only weakly correlated with the halo mass. Since the power-law relation is stiffer for the WHIM, the turbulent Mach number tends to increase with the mean temperature of the WHIM. This can be attributed to enhanced turbulence production relative to dissipation in particularly hot and turbulent clusters.